Physics
Scientific paper
Sep 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.188..871m&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 188, Sept. 1979, p. 871-881.
Physics
5
Coronal Holes, Energy Budgets, Solar Atmosphere, Solar Physics, Solar Wind, Atmospheric Models, Energy Requirements, Magnetohydrodynamic Waves, Momentum Transfer, Plasma Acceleration, Solar Magnetic Field
Scientific paper
Recent observations from spacecraft have established the correlation between high-speed solar wind streams in the vicinity of the earth, coronal regions of low density seen in the ATM coronagraph pictures, and coronal holes identified from X-ray photographs of the sun. Quantitative analysis of these data leads to the conclusion that most, if not all, of the solar wind originates in coronal holes and that it experiences the main part of its acceleration in the range between two and five solar radii. In this paper a simplified model is adopted to show that an adequate mechanism for the acceleration is the pressure applied to the solar atmosphere by the gradient of the momentum flux carried by Alfven waves travelling along the magnetic field lines. The total energy requirement of a coronal hole region is then estimated and this is shown to be significantly greater than for the other regions of the solar atmosphere.
Kopp Roger A.
McWhirter W. P. R.
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